Influence of the magnetic field topology in the evolution of small-scale two-fluid jets in the solar atmosphere

TL;DR

This study uses numerical simulations to analyze how magnetic field topology influences the evolution of small-scale two-fluid jets in the solar atmosphere, focusing on their dynamics, heat generation, and morphological characteristics.

Contribution

It introduces a detailed two-fluid MHD simulation approach to compare jet behavior in uniform and flux tube magnetic fields, highlighting subtle effects of magnetic topology.

Findings

Jets reach different heights depending on magnetic environment.

Velocity drift between ions and neutrals is minimal (~10^{-3} km/s).

Heat generated by ion-neutral friction is too small to heat the corona.

Abstract

We perform a series of numerical simulations to recreate small-scale two-fluid jets using the JOANNA code, considering the magnetohydrodynamics of two fluids (ions + electrons and neutral particles). We first excite the jets in a uniform magnetic field by using velocity pulse perturbations located at $y_{0}=$1.3, 1.5, and 1.8 Mm, considering the base of the photosphere at $y=0$ Mm. Then, we repeat the excitation of the jets in a magnetic field that mimics a flux tube. Mainly, the jets excited at the upper chromosphere ($y\sim1.8$ Mm) reach lower heights than those excited at the lower chromosphere ($y\sim1.3$ Mm); this is due to the higher initial vertical location because of the lesser amount of plasma dragging. In both scenarios, the dynamics of the neutral particles and ions show similar behavior; however, we can still identify some differences in the velocity drift, which in our simulations is of the order of $10^{-3}$ km s$^{-1}$ at the tips of the jets once they reached their maximum heights. Also, we estimate the heat generation due to the friction between ions and neutrals ($Q^{in}_{i,n}$), which is of the order of $0.002-0.06$ W m$^{-3}$; however it is small to contribute to the heating of the surroundings of the solar corona. The jets in the two magnetic environments do not show substantial differences other than a slight variation in the maximum heights reached, particularly in the uniform magnetic field scenario. Finally, the maximum heights reached by the three different jets are in the range of some morphological parameters corresponding to macrospicules, Type I spicules, and Type II spicules.